We present entropy distributions for a sample of galaxy
clusters from the Chandra public archive, which builds on
our previous analysis of nine nearby, bright clusters. By
studying the entropy distribution within clusters we
quantify the effect of radiative cooling, supernovae
feedback, and AGN feedback on cluster properties. This
expanded sample contains both cooling flow and non-cooling
flow clusters while our previous work focused only on
classical cooling flow clusters. We also test the
predictions of Mathiesen and Evrard (2001) by checking
whether the spectral fit temperature is an unbiased estimate
of the mass-weighted temperature, and how this estimate
effects the calculation of the intracluster medium mass.
Temperature and entropy maps for the clusters in our sample
using the Voronoi Tesselation method as employed by Statler
et al (in preparation) will also be presented. These maps
serve as a prelude to future work in which we will
investigate how well such maps may represent the "true"
projected quantities of a cluster by comparing deprojected
real and simulated clusters from our sample and the Virtual
Cluster Exploratory, respectively. Our discussion focuses on
tying together feedback mechanisms with the breaking of
self-similar relations expected in cluster and galaxy
formation models.